MNRAS 000, 000–000 (0000) Preprint 22 March 2019 Compiled using MNRAS LATEX style file v3.0
The O star hinterland of the Galactic starburst, NGC 3603
J. E. Drew1?, M. Mongui´o1, N. J. Wright2
1School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield AL10 9AB, UK 2Astrophysics Group, Keele University, Keele, ST5 5BG, UK
22 March 2019
ABSTRACT The very bright and compact massive young cluster, NGC 3603, has been cited as an example of a starburst in the Milky Way and compared with the much-studied R136/30 Doradus region in the Large Magellanic Cloud. Here we build on the discovery by Mohr-Smith et al.(2017) of a large number of reddened O stars around this cluster. We construct a list of 288 candidate O stars with proper motions, in a region of sky spanning 1.5×1.5 square degrees centered on NGC 3603, by cross-matching the Mohr- Smith et al. (2017) catalogue with Gaia DR2 (Gaia Collaboration et al. 2018). This provides the basis for a first comprehensive examination of the proper motions of these massive stars in the halo of NGC 3603, relative to the much better studied central region. We identify up to 11 likely O star ejections – 8 of which would have been ejected between 0.60 and 0.95 Myr ago (supporting the age of ∼1 Myr that has been attributed to the bright cluster centre). Seven candidate ejections are arranged in a partial ring to the south of the cluster core spanning radii of 9–18 arcmin (18–36 pc if the cluster is 7 kpc away). We also show that the cluster has a halo of a further ∼100 O stars extending to a radius of at least 5 arcmin, adding to the picture of NGC 3603 as a scaled down version of the R136/30 Dor region. Key words: stars: early-type, (Galaxy:) open clusters and associations: NGC 3603, Galaxy: structure, surveys
1 INTRODUCTION dense and massive clusters in the Milky Way. Indeed, the ex- treme stellar density in the core has prompted comparisons Massive young clusters are rare objects that nevertheless ex- with the extragalactic starburst phenomenon (e.g. Eisen- ert a major influence on their galactic environments. Their hauer et al. 1998; Moffat et al. 2002; Stolte et al. 2006). The modes of formation remain an important topic of research, mass of the cluster is among the highest measured in the echoing continuing significant uncertainty in the modes of Milky Way: Harayama et al.(2008) placed it in the range evolution of the most massive stars that are their distinctive from 10 000 up to 16 000 M , while Rochau et al.(2010) constituents. Clues to the early internal dynamics of massive obtained ∼18 000 M . The age often cited for NGC 3603, young clusters can come from the O stars they eject (Fujii & based on the stellar content of its inner core of diameter Portegies Zwart 2011). With the arrival of Gaia DR2 proper ∼ 20 arcsec is 1 to 2 Myr (e.g. Sung & Bessell 2004; Melena
arXiv:1903.09053v1 [astro-ph.SR] 21 Mar 2019 motions and the availability of wide field photometric sur- et al. 2008; Kudryavtseva et al. 2012). This core is some- veys, the opportunity now exists to locate ejected O stars times referred to as the HD 97950 cluster. Measurements in the environs of their birth clusters. In a previous paper over a wider sky area out to a radius of an arcminute or so, (Drew et al. 2018) we studied the example of Westerlund have indicated that an older, lower density population may 2 and discovered a surprisingly ordered ’twin-exhaust’ pat- be present as well (Melena et al. 2008; Beccari et al. 2010). tern of ejections that may favour the creation of Westerlund 2 via the merger of distinct sub-clusters. Here we move on In earlier work (Mohr-Smith et al. 2015, 2017, here- to the example of NGC 3603, the even brighter and more after MS-I and MS-II), we presented blue selections of OB compact clustering in the region. stars from the VST Photometric Hα Survey of the South- Like Westerlund 2, NGC 3603 is in the Carina region ern Galactic Plane and Bulge (VPHAS+, Drew et al. 2014) of the Galactic Plane. It is one of a small number of very across the Carina region, and showed that their conversion to spectroscopically-confirmed OB stars is very high. The MS-II list of 5915 O-B2 candidates is accompanied by high- ? E-mail: [email protected] quality measures of extinction, along with estimates of ef-
c 0000 The Authors 2 J. E. Drew et al fective temperatures that are good enough to broadly clas- sify as early-O, later-O and early-B stars. These are derived from fitting each object’s spectral energy distribution (SED) 150 as represented by its u/g/r/i/J/H/K magnitudes. Here, we reuse MS-II in order to focus on the hinterland of NGC 3603. This paper is organised as follows. First, we select from 100 MS-II a set of high-confidence O stars within a region of 1.5×1.5 sq.deg centred on NGC 3603, and crossmatch it with the Gaia DR2 database (Gaia Collaboration et al. 2018) with the aim of utilising the proper motion (PM) data (Sec- 50 tion2). We then compute the mean proper motion of the cluster using stars located within 1 arcminute of the cluster centre which becomes the basis for relative proper motions 0 (rPM, see sections 4.1 and 4.2). This enables the identifica- 4.2 4.3 4.4 4.5 4.6 tion of probable cluster escapes that turn out, intriguingly, log(Teff K) to be located in a half ring (section 4.3). After some sam- 140 ple decontamination, we consider the radial distribution of the O star candidates and find it largely follows the King 120 model adopted by Harayama et al.(2008). The paper ends with a discussion of the significance of the results and some 100 conclusions (sections6 and7). 80
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2 CONSTRUCTION OF THE SAMPLE 40 We adopt as the central reference position in the core of 20 NGC 3603 the Galactic coordinates, ` = 291◦.617, b = ◦ −0 .523. The selection box on the sky around this posi- 0 tion is a square occupying 1.5×1.5 deg2, with sides oriented 0 1 2 3 4 5 6 7 8 9 10 along the directions of constant Galactic longitude and lati- extinction (A0) tude. Within this region, the MS-II database provides a list of 1663 blue-selected OB candidate stars. Of these we retain 100 as a long list those objects for which the reported quality 2 of fits to their optical-NIR SEDs is χ < 25. MS-II recom- 80 mended a tighter χ2 limit than this for the selection of ”good
OB stars”: it is relaxed here so as not to exclude detected 60 objects close to the centre of NGC 3603 that are known al- ready to be early-type emission line stars. This reduces the list to 1537 objects. How these stars are distributed in terms 40 of best-fit effective temperature (or log(Teff K) as plotted) and extinction, A0, and 2MASS K magnitude is shown in 20 Figure1. We remind that A0 represents the monochromatic extinction at a wavelength of 5495 A.˚ 0 To focus the long list down onto the likely O star con- 6 7 8 9 10 11 12 13 14 K magnitude tent of the region at a distance D . 8 kpc, and extinction A0 . 10 magnitudes, we cut both on effective temperature Figure 1. These histograms show how the MS-II objects inside 2 2 such that log(Teff K) > 4.44 and on K magnitude such that the 1.5×1.5 deg box centred on NGC 3603, satisfying χ < 25, K < 13.0. The first cut admits objects with estimated effec- are distributed in effective temperature (top panel), extinction, tive temperatures greater than 27500 K: since O stars are A0 (middle) and K magnitude (bottom). The full sample of 1537 associated with effective temperatures exceeding ∼30000 K, stars is shaded in blue. The green bars pick out the selection with this builds in some margin for fit error. The reasoning be- logTeff > 4.44 and K < 13.0 mag. These are the focus of this study. hind the second cut is that, since MK ' −3 for an O9.5 main sequence star (Martins et al. 2005), such a star at a maximal distance of 8 kpc, with A0 = 10, would suffer no more than ∼ 1 magnitude of K extinction, resulting in an apparent magnitude of K ∼ 12.5. Setting the fainter limit of K = 13.0 again makes some allowance for error. How the up at position offsets ranging from ∼0.03 to ∼0.2 arcsec reduced sample compares with the full list from MS-II is (with a mean of ∼ 0.1 arcsec). The astrometry is ”good” in illustrated in Figure1. that all of them pass the mission-recommended test of as- Next, a cross-match of the reduced list of 325 stars with trometric quality: that the renormalised unit weight error, p 2 the Gaia DR2 catalogue was undertaken. We found that u/u0(G, BP − RP ) < 1.4, where u = (χ )/(N − 5) and 292 objects with good astrometry were successfully matched u0(G, BP − RP ) is the magnitude- and colour-dependent
MNRAS 000, 000–000 (0000) The O star hinterland of NGC 3603 3
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Figure 2. The on-sky positions of the 288 selected objects in the region around NGC 3603. The background image is constructed from VPHAS+ Hα data.
reference value.1 The minimum number of Gaia satellite vis- concern that there will be ’contamination’ due to objects ibility periods per source is 13, while the median value is 18. located in the first crossing of the Carina Arm at a distance As might be expected, given the centering of the Gaia G of 2–3 kpc (with NGC 3603 in the second crossing at > 6 transmission in the red part of the optical spectrum, the kpc, see section3). A sign of this in Figure2 is the pres- typical difference between MS-II r and Gaia G magnitudes ence of the bright nebula, NGC 3576, around ` ' 291◦.2, per source is modest, being in the region of 0.1-0.2 mag. b ' −0◦.65. This is known to be associated with the near The apparent magnitudes of the selection fall mainly in the Carina Arm (de Pree et al. 1999, give a distance of 3.0±0.3 range, 12.0 < r, G < 17.5. kpc). Accordingly we could anticipate some of the scatter of Finally, we removed 4 objects that are likely to be well objects in the vicinity of this nebula to be near-arm stars. into the foreground of NGC 3603 – specifically, stars with However the visual extinctions of the exciting stars of > 5σ Gaia DR2 parallaxes for which distances of under 4 NGC 3576 itself are high at over 10 magnitudes (Figuerˆedo kpc are indicated. This leaves 288 candidate O stars of which et al. 2002) while the known OB stars in its vicinity are too 15 are already in the literature. In the online appendix, a bright to appear in our sample (e.g. EM Car, an O8V+O8V table of names, positions and other important quantities is binary, V = 9.54). Furthermore, only 15 of the 288 stars has provided. This is our sample. How it is distributed on the A0 < 4 – for which a distance of under ∼4 kpc would be sky is shown in Figure2. implied if A0 were to rise with distance at a rate of 1 mag The absence of candidate O stars towards higher Galac- kpc−1 (see the discussion in section 5.3 of MS-II). We con- tic longitudes and more negative latitudes apparent in fig- clude that the amount of near-arm contamination – which ure2 is real, in the sense that the MS-II source catalogue would most likely be dominated by B stars – is well under only found cooler B stars in this corner (along with 4 inde- 10 percent. terminate objects returning unacceptably high χ2 SED fits). Another prominent feature of the emerging distribution is the dense, extended core of objects around the cluster po- 3 THE DISTANCE TO NGC 3603 sition. It is a reasonable first conjecture that most of the objects are associated with NGC 3603: within 2 arcminutes It is widely accepted that NGC 3603 is located in the far, of our fiducial position there are 56 O-star candidates, rising rather than the near, Carina Arm. Melnick et al.(1989) to 115 inside a radius of 8 arcminutes. presented and analysed UBV photometry of 74 stars over Within the field under consideration there could be a a region of ∼9 square arcminutes, determining a distance modulus of 14.3 (or D = 7.24 kpc). Sung & Bessell(2004) focused mainly on the inner region within 1 arcminute of the 1 See the Gaia mission document, GAIA-C3-TN-LU-LL-124-01 cluster centre and used dereddened VI photometry of stars by L. Lindegren to deduce a distance modulus of 14.2 ± 0.2 (or D = 6.9 ± 0.6
MNRAS 000, 000–000 (0000) 4 J. E. Drew et al
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5 0 4000 6000 8000 10000 12000 14000 distance in parsecs -0.56 4 291.64 291.62 291.60 291.58 Figure 3. The histogram of distances inferred from Gaia DR2 Galactic Longitude (deg) parallaxes for the 288 selected O-star candidates, using an EDSD prior with scale length of 1.5 kpc. Every parallax was increased Figure 4. A zoom into a 5 × 5arcmin2 box around the centre by 0.03 mas to allow for the known Gaia DR2 global offset. The of the cluster (it contains 69 stars). Because of the extreme con- blue histogram bars represent the entire sample. The grey bars fusion in the stellar core as imaged from the ground, no object are the distribution obtained on limiting the selection to stars lies within 12 arcsec of the centre, which is marked with a plus within 5 arcmin of the cluster fiducial position, while the green symbol. The 29 stars within a radius of 1 arcmin that were used colour picks out stars within 1 arcmin. to determine the mean cluster proper motion are encircled. All objects are coloured according to extinction. kpc). Since then Melena et al.(2008) have argued for D = 7.6 kpc, based on a spectrophotometric analysis of mainly respectively – i.e. scarcely different from, if a little lower than cluster O stars. Usefully, these authors also provided two the means. tables summarising stellar and kinematic distances in the This pattern is plausible even if the numerical values literature prior to their work (see their Tables 4 and 5). A of the distances are subject to a presently undetermined kinematic measure not included in this compilation was that systematic error (capable of shifting the means by more than by N¨urnberger et al.(2002) based on CS line observations: 1 kpc either way). We would expect the MS-II catalogue they obtained D = 7.7±0.2 kpc, from CS velocities of 14.2± to provide more candidates in the foreground of NGC 3603 1.6 km s−1 (LSR). The emergent picture from the literature than in the increasingly reddened background, resulting in a is that since the mid 1980s most estimates have ranged from bias toward a shorter distance in the largest sample. This is 6 kpc up to 8 kpc. Here, we will work with D = 7 ± 1 kpc. present, but it is not strong as it only indicates a difference in A distance of 7 kpc to NGC 3603 implies an astromet- the mean of around 1 kpc (∼ 15 percent) between the stars ric parallax of 0.143 mas would be measured in the ideal in the wider environment and those in the cluster centre. case of negligible error. The Gaia DR2 results are known Qualitatively, the outcome of this exercise is not sen- to exhibit an offset of -0.03 mas, and a position dependent sitive to the EDSD scale length prior: for example, if it is systematic error of up to 0.1 mas (Lindegren et al. 2018). doubled to 3 kpc there is again a gradual rise in the mean In this situation, we should not expect Gaia DR2 parallax distance estimate as the sky area sampled is focused more data to do more than perhaps statistically corroborate ex- onto NGC 3603. isting measures of distance. Figure3 shows the distribution of distances for our sample of 288 stars inferred on applying the EDSD (exponentially-decreasing space density) prior de- 4 RESULTS scribed by Luri et al.(2018): a scale length of L = 1.5 kpc 4.1 The proper motion of the core of NGC 3603 was adopted and 0.03 mas was added to each parallax to correct for the global Gaia DR2 offset. There are 30 cross-matched stars with astrometry, accepted Evidently the distribution in Figure3 is very broad. into the sample, that lie within 1 arcminute of our fiducial This remains true when the selection is limited to those close position (see Figure4). But none are closer to the nomi- to cluster centre. This is unsurprising in itself. What is of nal centre than 0.2 arcmin, as a consequence of the severe more interest is the trend in the mean and median measures source confusion in the brilliant cluster core typically seen in as the sample is reduced from the full set to, first, projected ground-based images. After one evident outlying object with separations from the centre of < 5 arcmin, and then to < 1 a high relative proper motion is removed from the subset, the arcmin. The changes are in the sense of increased mean, or remaining 29 stars yield a mean PM in Galactic co-ordinates −1 median, distance as the sky area is restricted: the means and of µ`,∗ = −5.881 ± 0.151 mas yr , and µb = −0.209 ± 0.151 formal errors from the distributions are mas yr−1. A check against the 6 Gaia DR2 objects, with no excess astrometric noise located closer to cluster centre, are • full sample: D = 7.2 ± 0.1 kpc (288 stars), consistent with this measure. • within 5 arcmin of centre: D = 7.6 ± 0.2 kpc (93 stars), At a distance of ∼ 7 kpc, the implied mean transverse • within 1 arcmin of centre; D = 8.2 ± 0.4 kpc (30 stars). motion in the b coordinate is equivalent to ∼7 km s−1, di- The medians for these three samples are 7.2, 7.5 and 8.1 kpc rected below the plane. This fits with what we would expect
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20 0
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latitudinal relative PM (mas/yr) -1
0 -2 -1 0 1 2 0 2 4 6 8 10 12 14 longitudinal relative PM (mas/yr) Impact parameter (arcmin) 50 Figure 6. The distribution of computed impact parameters (pro- jected nearest approach to cluster centre) up to 15 arcmin. The bars are overlaid to pick out different ranges in magnitude of 40 proper motion as follows: blue admits all values; grey signifies −1 objects with |PMr| > 0.2 mas yr ; magenta, |PMr| > 0.4 mas yr−1, pink, |PM | > 0.6 mas yr−1. 30 r N
20 yr−1, appears consistent with the Hubble Space Telescope (HST) results of Rochau et al.(2010) and Pang et al.(2013) based on somewhat fainter intermediate mass stars. Rochau 10 et al.(2010) obtained an intrinsic 1-D dispersion from 234 stars inside a radius of ∼ 0.25 arcmin of 0.141±0.027 mas −1 0 yr . Pang et al.(2013) considered the same region and -2 -1 0 1 2 a similar scale of sample and measured 0.146±0.016 and longitudinal relative PM (mas/yr) 0.198±0.016 mas yr−1 in two orthogonal directions.
Figure 5. The proper motions of the retained sample of objects relative to the core of NGC 3603 in mas yr−1. In the upper panel, the 29 stars within 1 arcmin of the cluster centre used to compute 4.2 Proper motions of the wider sample the cluster PM are shown in green. Stars in grey have relative proper motions of magnitude less than 0.3 mas yr−1 – they can be Proper motions relative to the mean cluster value, PMr, seen as commensurate with those typifying the core region. 62% of have been computed and are shown in the upper panel of the sample (180 stars) fall in this group. The 9 objects in pink are Figure5. There is evidently a tight clustering around the candidate ejections with relative PMs exceeding 0.6 mas yr−1 and origin that is similar in dispersion to the ’core’ objects. Set- trajectories passing within 1 arcmin of the centre of NGC 3603. ting an upper bound on the magnitude of the PMr of 0.3 All other stars are in blue. The lower panel is the histogram of the mas yr−1, there would be around 93 qualifying objects that longitude component of the relative PM for all objects (in blue). lie within 10 arcmin of cluster centre – with another 87 with Notice the double-peaked character of the longitude distribution similarly low PMr scattered across the wider field. An im- and the negative shoulder showing between −0.4 and −0.8 mas portant consideration here is whether a small relative proper yr−1. For comparison the distributions obtained on limiting the motion implies proximity and/or dynamical association with selection to within 5 arcmin (grey) and 1 arcmin of cluster centre (green) are superposed: the shoulder and double-peaking weaken NGC 3603. For some, especially those at modest angular dis- and disappear. placements from the cluster, this is likely and credible. But we should not forget the other option that some candidate objects are foreground or background and merely tracing Galactic rotation: a distance change of ∼1 kpc in- if this massive young cluster has negligible vertical motion: duces a longitudinal proper motion change of just ∼0.2 mas the observed µ should then be equal to and opposite in b yr−1 (depending somewhat on choice of rotation law). There sense to the Sun’s motion – which has indeed been found is evidence this could be happening, as shown in the lower to be +7 km s−1 to within one significant figure (see e.g. panel of Figure5: the distribution in the relative PM longi- Sch¨onrich et al. 2010). tude component verges on double-peaked and shows a neg- It is also encouraging that the dispersion around the ative shoulder that may signal the mixing in of a higher- mean we obtain in both coordinates, of 0.151±0.0202 mas PM foreground population. When the sample is limited to those within a few arcminutes of the core, the skew and 2 tendency towards double peaking reduces and the shoulder The√ uncertainty is obtained by dividing the standard deviation by 2N − 2 where N = 29. disappears.
MNRAS 000, 000–000 (0000) 6 J. E. Drew et al
4.3 Candidate ejections put forward by Roman-Lopes et al.(2016) is their relative proper motion significant (the largest is 0.178 ± 0.020 mas For the present purpose of initial classification, we note that yr−1, obtained for RFS 1). In the case of RFS 8, some 29 at a distance of 7 kpc, a proper motion magnitude of 0.6 arcmin away from the cluster centre, runaway status is en- mas yr−1 corresponds to an in-sky or tangential speed of 20 −1 tirely ruled out as the implied timescale since ejection would km s . We will regard any object that exceeds this thresh- have to exceed 10 Myr. RFS 1 and 2 are respectively only old as meeting the first of two criteria required of candidate 0.7 and 1.0 arcmin away from cluster centre, leaving open ejections from NGC 3603. 38 objects qualify in this regard. the possibility of ejection should spectroscopic observations The second criterion to be satisfied is that the trajectory of reveal significant relative radial velocity. motion needs to have an impact parameter (closest distance . of approach to NGC 3603 centre) under 1 arcmin, and the The on-sky pattern traced by the group of 7 is strikingly sense of motion needs to be away from the cluster. a half ring to the south of the core region. The one object, Figure6 shows how the stars with impact parameter #14172, sitting outside this zone also distinguishes itself in less than 15 arcmin break down according to magnitude Table1 as the only candidate with an estimated time of of proper motion. Among the 199 stars plotted there is a flight appreciably larger than 1 Myr. Otherwise, the clear clear peaking of impact parameter to smaller values (irre- norm is a flight time of under 1 Myr. In section6 we will spective of relative PM magnitude). This pattern persists as consider what this tidy pattern of ejections may signify. the total list is reduced by cutting on an increasing mini- mum relative PM magnitude. In the most extreme group, −1 with |PMr| > 0.6 mas yr , 9 out the 38 stars have an im- 4.4 Other high relative proper motion objects in pact parameter of under 1 arcmin. These are our candidate the region ejections meeting the first two criteria. They are coloured Figure6 shows that there are high relative PM stars in the lighter pink in Figure5, while their on-sky distribution is sample with trajectories that do not pass close to the clus- shown in7. Important properties for this set of objects are ter centre. These will be the stars shown in light pink and given in Table1. magenta, at impact parameters exceeding 1 arcmin. In par- Of the 9 candidates, 1 object (VPHAS-OB1-13519, or −1 ticular there is a group of fast (|PMr| > 0.6 mas yr ) ’near #13519 in Table1) is a relevant inclusion in that |PMr| = misses’ with impact parameters up to 4 arcmin, which are −1 0.886 ± 0.068 mas yr is well above threshold for the first worth brief consideration (their properties are in Table2). criterion – otherwise, it is located within 1 arcmin of cluster The uncertainties on the impact parameters of 2 of them are centre, and so must have an impact parameter < 1 arcmin. large enough that it cannot be ruled out that they may have The direction of its PMr is almost opposite to that it would been ejected from within 1 arcmin of the cluster centre. For have if merely a foreground contaminant. #13519 could be this reason they have been included in Figure7 and coloured a very early-stage ejection, exiting the central region at a in blue. One of the two, #13280, may continue the ring of −1 tangential speed of ∼ 30 km s (at 7 kpc) ejections discussed above in section 4.3. The other, #13452, More interest attaches to the group of 7 separated from represents a contrast in that it is much further away from the cluster centre by between 9.68 and 17.56 arcmin. Repre- NGC 3603 and would have to have been ejected about 3 sentative values for the impact parameter and error in this million years ago if indeed it was ejected. group are respectively ∼0.3 and ∼1 arcmin (see Table1)– The status of the remaining 5 objects in Table2, that implying that our second criterion may actually scoop up appear never to have been in the cluster core, is less certain. stars originating from within a radius of ∼ 1.3 arcmin. At There is a case to be made that one of them, #13708, is the shortest radius in this group, the probability of a star in fact a foreground star in that its Gaia DR2 parallax is having the right direction of travel to satisfy the second cri- 0.3297 ± 0.0731, a 4.5σ measurement. It has only remained terion (if all directions of travel are equally likely) is 0.043. in the sample because the 5σ limit is not breached – indeed The probability that it also has |PMr| > 0.6 is empirically it is the object with the highest measured parallax retained 38/288 ' 0.13. Hence the total combined chance is ∼0.006. and it is responsible for the lowest occupied histogram bin For the most far-flung member of the group, at almost twice in Figure3. the radius, the probability essentially halves. This general We can try a combination of high relative PM and high level of individual probability hints that perhaps one of the impact parameter as the means to identify ’contaminant’ seven objects could be a false positive (given the total pop- objects. We view it as improbable that higher relative PM −1 ulation drawn from). stars (|PMr| > 0.42 mas yr , or > 2σ in the 2-D disper- One of the group of 7 has already been identified sion), with impact parameters larger than some minimum as a likely ejection by Gvaramadze et al.(2013): it is value are associated with the cluster. Anticipating the result 2MASS J11171292-6120085, an O6V star with an associated of the next section, we look for impact parameters exceeding suitably-offset bow shock. In MS-II it is VPHAS-OB1-13931 6 arcmin. Such a cut pulls out 30 objects. It is interesting (#13931 in Table1). It is located nearly 16 arcmin from the to note that 20 in this group have significantly negative lon- −1 −1 centre of NGC 3603 and its relative PM is 1.58 mas yr gitudinal |PMr| (< −0.4 mas yr ) – a property consistent (or ∼52 km s−1 at 7 kpc). It is the object almost directly to with being in the foreground to the cluster. Indeed, these the left of cluster centre in Figure7. However, its proposed objects dominate the negative ’shoulder’ seen in Figure5 partner object, WR 42e, displaced to the opposite side of (lower panel), and all are at an angular separation of at the core of NGC 3603 is not supported as an ejection: its least 20 arcmin from the centre of NGC 3603. The remain- |PMr| is small at 0.125±0.034 mas/yr. Similarly, for none ing 10 stars are – with one exception only – over ∼30 arcmin of the three additional ejection candidates, RFS 1, 2 and 8, distant. The exception is #13390 that is at a radius of 9.1
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Table 1. Proper motions and related quantities for stars meeting the first two criteria for ejection from the centre of NGC 3603. Column 1 specifies the MS-II catalogue number. The Gaia DR2 proper motions appear in columns 2 and 3. Column 4 is the angular distance in arcminutes from the fiducial position ` = 291◦.617, b = −0◦.523. Columns 5 and 6 give the proper motion relative to the core-region mean, PMr, in Galactic coordinates. Column 7 is magnitude of the relative proper motion, while column 8 gives the trajectory impact parameter (in arcminutes). The (distance-independent) travel time from the fiducial position is in column 9.
MS-II Proper motion Radius Relative PM, PMr |PMr| IP Travel time Note # µα,∗, µδ mas/yr arcmin ∆µ`,∗, ∆µb mas/yr mas/yr arcmin Myr 13362 −6.400±0.031 1.880±0.030 9.68 −0.766±0.043 −0.362±0.040 0.847±0.021 0.27±0.62 0.69 13436 −6.167±0.053 1.315±0.044 12.09 −0.343±0.061 −0.803±0.052 0.874±0.027 0.28±1.05 0.83 13519 −6.072±0.133 2.660±0.116 0.73 −0.743±0.145 0.484±0.108 0.886±0.068 0.13±0.14 0.05 13804 −5.444±0.132 0.871±0.114 17.03 0.492±0.139 −0.955±0.113 1.074±0.059 0.57±2.77 0.95 13860 −4.677±0.080 2.105±0.075 12.67 0.759±0.083 0.473±0.083 0.894±0.042 0.02±1.61 0.85 13908 −4.712±0.062 0.990±0.056 15.58 1.130±0.069 −0.578±0.062 1.270±0.034 0.79±1.06 0.74 13918 −4.584±0.060 0.646±0.053 17.56 1.375±0.067 −0.852±0.059 1.618±0.032 0.30±0.92 0.65 13931 −4.050±0.060 1.459±0.054 15.81 1.577±0.067 0.099±0.061 1.580±0.033 0.25±0.65 0.60 a 14172 −4.924±0.035 1.925±0.036 30.59 0.593±0.043 0.216±0.047 0.631±0.022 0.02±2.87 2.91 a: this is 2MASS J11171292-6120085 (Gvaramadze et al. 2013)
Table 2. Proper motions and related quantities for stars with impact parameters between 1 and 6 arcmin, and high relative PM (> 0.6 mas yr−1). The columns are as in Table1. Note that a timescale is only given in the final column if the uncertainty on the impact parameter leaves open the possibility that the star may have originated inside a radius of 1 arcmin around the cluster centre.
MS-II Proper motion Radius Relative PM, PMr |PMr| IP Travel time Note # µα,∗, µδ mas/yr arcmin ∆µ`,∗, ∆µb mas/yr mas/yr arcmin Myr 13280 −6.309±0.072 3.156±0.071 16.09 −1.144±0.076 0.860±0.078 1.431±0.038 2.06±1.20 0.67 13377 −5.636±0.042 2.736±0.036 24.36 −0.364±0.050 0.713±0.046 0.801±0.023 3.48±1.97 13452 −5.359±0.036 2.870±0.033 43.88 −0.155±0.045 0.939±0.044 0.951±0.022 3.25±2.38 2.77 13573 −5.384±0.119 1.324±0.095 2.60 0.383±0.126 −0.511±0.094 0.639±0.053 1.81±0.45 13708 −6.518±0.130 1.093±0.120 2.70 −0.590±0.129 −1.138±0.127 1.282±0.064 2.59±0.10 b 13766 −6.460±0.068 1.986±0.065 5.52 −0.860±0.072 −0.285±0.072 0.906±0.036 3.12±0.46 14359 −6.377±0.044 1.890±0.040 40.68 −0.748±0.051 −0.344±0.050 0.823±0.026 3.69±3.28 c b: this star narrowly missed exclusion on account of large parallax – see text c: the relative proper motion of this star is directed towards the cluster
+00.25° N
#13452 E
+00.00°
-00.25°
#14172 #13280 #13860
Galactic Latitude NGC 3603 -00.50° #13931 #13519
#13362 #13908
#13918 -00.75° #13436 #13804
292.00° 291.50° 291.00° Galactic Longitude
Figure 7. The on-sky distribution of the O-star candidates, with relative proper motion magnitude exceeding 0.6 mas/yr. Objects coloured in red are those with impact parameters that are < 1 arcmin (Table1). The two objects in blue are from Table2: they have impact parameter errors that allow a trajectory consistent with ejection at reduced probability.
MNRAS 000, 000–000 (0000) 8 J. E. Drew et al arcmin, with an estimated impact parameter of 6.5 arcmin: The lower panel of Figure8 provides some corroborating it is an IR-bright object (K = 9.71) that also happens to insight into what is going on – essentially, the dependence be highly obscured (A0 = 9.84 mag). Potentially, it is in the of O-star extinction on radius is orderly and in keeping with background to the cluster. the earlier mapping to ∼4 arcmin of colour excess by Sung & Bessell(2004). But from around 6 arcmin, outwards, the order begins to break down and a number of O stars begin to present with lower extinction relative to the trend seen at 5 THE O STAR HINTERLAND shorter radii. This could well be foreground contamination The size of region on the sky that should be associated with revealing itself. NGC 3603 is challenging to define. Based on Ks photometry, We conclude that the ’halo’ of NGC 3603 may very N¨urnberger et al.(2002) constructed a stellar surface density well extend beyond 5 arcmin, and that essentially all the O map to a range of limiting magnitudes and concluded that stars drawn from the MS-II catalogue inside this radius are at a radius of 2.5±0.25 arcmin a mean field takes over from associated objects. Out of the 100 objects inside 5 arcmin, a declining cluster density profile. A King model was fit to just 15 were mentioned in the literature prior to MS-II (their the data, in which the core and tidal radii were respectively names are matched to the MS-II and Gaia DR2 identifiers 23 and 1300 arcsec. This has been revisited by Harayama in table A1). The lower panel of Figure8 demonstrates that et al.(2008), using NIR adaptive-optics data better able to most are expected to have effective temperatures of ∼35 kK resolve the core. They revised the core radius down to 4.8 or more – implying masses exceeding ∼20 M (see Ekstr¨om arcsec, and proposed a tidal radius of 1260 arcsec (21 ar- et al. 2012). cmin) on general dynamical grounds. The latter is much the same as the N¨urnberger et al.(2002) estimate. Importantly, Harayama et al.(2008) elaborated the evidence in favour of 6 DISCUSSION significant mass segregation such that the bright core con- 6.1 The pattern of O-star ejections tains a relative concentration of the most massive (O) stars – a result that was later reinforced by Pang et al.(2013). Our selection and survey of O-star proper motions relative to Because we have a honed selection of O stars, across NGC 3603 has revealed at 9 credible ejections (Table1) and a wide field, we have the opportunity to review the radial 2 further less certain examples (Table2). The scale of the density profile, restricted to the context of the most massive measured proper motions for all but two of the candidates stars for which the enveloping ’field’ density would most indicates a time since ejection of under a million years. This likely be low. is entirely congruent with findings that the bright compact We have determined the density profile out to a max- centre of the cluster, contained inside a radius of 1 arcmin, is imum radius of 20 arcmin, supplementing the Gaia DR2 no older than 1–2 Myr (e.g. Sung & Bessell 2004; Kudryavt- cross-matched list with 17 objects in our initial selection seva et al. 2012). Indeed our result endorses this young age, that so far lack matches – this adds, as a crude average, one and carries no dependence on the still uncertain distance to object per bin. We leave out #13390 and #13708 (see sec- NGC 3603. tion 4.4). The resultant profile is shown in the upper panel The two objects with trace-back times closer to 3 Myrs of Figure8. As a comparison, the King model proposed by (#14172 and, with less precision, #13452) may be evidence Harayama et al.(2008) is shown rescaled to coincide with of an earlier phase of star-forming activity. Or they might the measured density in the radius range 1.0 – 2.0 arcmin. not survive further scrutiny. We note now that their extinc- Two features stand out. First, the model rolls off a little tions are relatively low at respectively A0 = 4.31 and 4.40 – quickly relative to the observed O stars, possibly indicating to be compared with 5 < A0 > 8 for all the ejections in the too short a tidal radius. If instead the tidal radius is set to last 1 Myr. To pursue this question further requires expand- be very large (cyan points in the plot), the match is better ing the search area to pick up more fast-moving ejections but high given that some contaminating objects almost cer- (#13452 is right on the edge of our 1.5 × 1.5 sq.deg region), tainly remain present. Second, over the radius range 0.2 to and/or follow-up spectroscopy to better characterize these 1 arcminute, the King-model trend is relatively underpopu- objects. lated. Given that the count of O stars inside 0.2 arcmin is The most remarkable feature of the on-sky arrangement most likely an underestimate (see Melena et al. 2008), this of the candidate ejections is that the 7 most convincing are could be a reflection of the mass segregation described by arranged in a semi-oval emphasising the south side of the both Harayama et al.(2008) and Pang et al.(2013) that is cluster core (Figure7). At most, one of these might be a most evident inside a radius of 0.5 - 1 arcmin. false positive. An eighth (#13280) helps to spread the pat- The King model superposed in Figure8 works quite well tern a bit more into the north but it is more marginal for in- with minimal contamination out to a radius of ∼ 5 arcmin. clusion since its impact parameter is a factor of a few larger. At larger radii it becomes necessary to consider a sliding Statistically there are no grounds to suspect that a bias in scale of options ranging from a lot of presumed field contam- the sample as a whole, favouring the south over the north, ination combined with the fall-off predicted by Harayama et shapes this – the main difference is that north of cluster cen- al.’s (2008) King model, through to a little contamination on tre the density of objects drops away more quickly than to- top of a distribution subject to a larger a tidal limit. If the wards the south. There is no reason to suspect a north-south tidal radius is ∼ 21 arcmin, then the O star count predicted extinction bias either (see the extinction maps of Marshall by the rescaled King model, outside a radius of 0.2 arcmin, et al. 2006; Planck Collaboration et al. 2014). The simplest is ∼138 – we count 100 to 5 arcmin, 132 to 10 arcmin, and option is to accept, provisionally, that the pattern reflects a 166 to 20 arcmin. reality beyond mere coincidence.
MNRAS 000, 000–000 (0000) The O star hinterland of NGC 3603 9
10
100 4.62 9 4.60
10 ) g
a 8 4.58 m (
1 0 A
4.55
n 7 o i logTeff t
0.1 c 4.52 n i t
x 6
e 4.50 O density per sq.arcmin 0.01 5 4.47
0.001 4.45 4 0.1 0.5 1 5 10 15 20 0.1 0.5 1 5 10 15 20 radius (arcmin) radius (arcmin)
Figure 8. On a log-log scale, the upper panel shows the density of selected O stars as a function of radius out to 20 arcmin (red circles). The error bars are Poissonian. The O star count inside 0.2 arcmin is equated to the number visible in Figure 2 of Melena et al (2008): it is likely to be a lower limit. The blue data points trace the King profile obtained by Harayama et al (2008), while the cyan points show the same profile computed for a very large tidal radius. Both model curves have been rescaled to match the O star density in the 1.0-2.0 arcmin bin. The lower panel shows the radial extinction distribution for comparison, with the data points coloured according to the MS-II effective temperature estimate.
The pattern seen is in striking contrast to the also- could be linked to an event 0.75±0.11 Myr ago. However orderly pattern of ejections from Westerlund 2 (Drew et al. the propagated errors on the individual timescales do not 2018): in that case a distinctly linear pattern was present exceed ∼0.05 Myr (if we assume the point of origin within with ejections located on either side of the cluster. It was ar- the cluster for each ejection is unknown to within 0.2 ar- gued that sub-cluster merging to produce present-day West- cmin). Hence, a modest spread in time of ejection of up to erlund 2 could be responsible for the preferred axis of the ∼200,000 years appears more likely. To make progress, ra- ejections. Could something similar be involved here? dial velocities for the candidate ejections would be a good Fukui et al.(2014) have presented detailed CO obser- next step as this would build a better view of the full three- vations in the vicinity of NGC 3603, and have deduced dimensional geometry. It is possible that the projection into from them evidence of a cloud-cloud collision that took two dimensions exaggerates the degree of coherent spatial place around a million years ago. And they made a link organisation present. between NGC 3603 and Westerlund 2 as two examples of A last point of interest is that Figure7 and the data ’super star clusters’ – suggesting that this status owes some- in Tables1 and2 indicate that there are potentially two thing to cloud-cloud collisions. In this context we note that ’pairings’ of ejections: #13280 may pair with either #13908 the most massive molecular cloud component (reported by and #13918, while #13362 and #13860 are moving in close Fukui et al. 2014), implicated in the case of NGC 3603, is to opposite directions. This leaves 3 (or 4) of the stars in the centred on ` = 291◦.58, b = −0◦.42. This is 5–6 arcmin ring of ejections without evident partners – one of these is north of the core of NGC 3603 and, in the plane of the sky, #13931 for which a partner has been claimed (Roman-Lopes on the opposite side to the semi-circle of ejections. If this et al. 2016), but has only a small proper motion. cloud carried most of the momentum in the putative colli- sion, we might anticipate that most of the ejections would appear on the same side (contrary to what is seen). 6.2 The significance of the O star halo From a theoretical perspective, the formation of NGC We noted in the introduction that much of the work to date 3603 has been discussed in terms of a monolithic process – on NGC 3603 has focused on the inner ∼arcminute around either as a single intense star-forming event (Banerjee & the brilliant cluster core. In this study, encouraged by the Kroupa 2014) or via the prompt assembly of a compact initial findings reported by MS-II, we have expanded the group of sub-clusters (Banerjee & Kroupa 2015). The for- area examined up to over a square degree. With the support mer is favoured by (Banerjee & Kroupa 2015) and resembles of Gaia DR2 proper motions, the case has been built for an the early assembly concept discussed by Fujii & Portegies extensive hinterland of associated O stars that persists to at Zwart(2013). Dynamical stellar ejection is the only rele- least a radius of 5 arcmin. The distribution is consistent with vant ejection process here, for the reason that the youth of Harayama et al’s (2008) preferred King model, for which NGC 3603 should mean no supernovae have exploded yet. a tidal radius of 21 arcmin was adopted. Harayama et al. In this context, there need be no particular expectation of (2008) pointed out that the tidal radius is hardly constrained a particular pattern of ejections: random vectors, but on a at all and could be even larger. The clear implication is that timescale comparable with the formation event would seem a number of the O stars in our sample between ∼5 and ∼20 plausible. The times since ejection for all objects making up arcmin could be halo members too. It will take full space the ring fall within a quite narrow range, from 0.60 to 0.95 motions to clarify this. Myr. Expressed as a mean and standard deviation, the ring It has been mooted before that NGC 3603 might be a
MNRAS 000, 000–000 (0000) 10 J. E. Drew et al
Galactic counterpart to R136 in the 30 Doradus region of Large Magellanic Cloud, albeit scaled down to around 40% the LMC. In pursuit of this point, Melena et al.(2008) ar- of the total O-star population. gued that R 136, the central cluster of 30 Doradus, contains Appendix B (online only) provides the derived relative between 1.1 and 2.4 times as many very high mass stars proper motion data forming the basis of this study, as ta- (Mbol < −10) as found in the core of NGC 3603 – that is, ble B1. the scale factor is not so large. We now make essentially the same comparison, basing it on the wider environment rather than the core region. Evans ACKNOWLEDGEMENTS et al.(2011) list 100 stars with KS < 15.5 (MK < −3 or Mbol < −6.8) in the annulus between 0.2 to 1 arcmin, reach- Use has been made of data products from the Two Micron ing out into R 136’s ’halo’. This can be compared with the All Sky Survey, which is a joint project of the Univer- count here to the same MK limit, in the equivalent angular sity of Massachusetts and the Infrared Processing and range, after rescaling for the much shorter distance to NGC Analysis Center/California Institute of Technology, funded 3603 of 7±1 kpc (with R136/30 Dor at a distance of 50 kpc, by the National Aeronautics and Space Administration the rescale is 7×, giving an angular radius range of 1.4 to 7 and the National Science Foundation. This work has arcmin). The analogous count is ∼40, implying a scale-down also used data from the European Space Agency mission from R136/30 Dor by about a factor of ∼2.5. This is at the Gaia (https://www.cosmos.esa.int/gaia), processed by the upper end of the Melena et al.(2008) range, and is just Gaia Data Processing and Analysis Consortium (DPAC, about compatible with it. But we have to differ with their https://www.cosmos.esa.int/web/gaia/dpac/consortium). conclusion (and that of Moffat et al. 2002) that there is ”no Funding for the DPAC has been provided by national surrounding massive halo of cluster stars”. There evidently institutions, in particular the institutions participating in is. The difference between then and now is the availability the Gaia Multilateral Agreement. of calibrated wide field multi-colour photometry. Much of the analysis presented has been carried out via TopCat (Taylor 2005). JED and MM acknowledge the support of a research grant funded by the Science, Technology and Facilities Council of the UK (STFC, ref. ST/M001008/1). NJW ac- 7 CONCLUSIONS knowledges receipt of an STFC Ernest Rutherford Fellow- The crossmatch we have carried out of 288 stars in the hin- ship (ref. ST/M005569/1). We thank the referee of this pa- terland of the massive young cluster, NGC 3603, of high- per for helpful comments. purity O-star candidates in MS-II and the Gaia DR2 release has had two main outcomes. 1. Our appraisal of the relative proper motions has re- REFERENCES vealed up to 11 candidate O star ejections. Nine of these have been ejected within the last one million years. Indeed Banerjee S., Kroupa P., 2014, ApJ, 787, 158 the timescale spread is limited to 0.6–0.95 Myrs for eight Banerjee S., Kroupa P., 2015, MNRAS, 447, 728 Beccari G., et al., 2010, ApJ, 720, 1108 of them. This lends clear support and an interesting datum Drew J. E., et al., 2014, MNRAS, 440, 2036 to earlier photometric studies that have argued the central Drew J. E., Herrero A., Mohr-Smith M., Mongui´oM., Wright cluster is no more than 1–2 Myrs old (Sung & Bessell 2004; N. J., Kupfer T., Napiwotzki R., 2018, MNRAS, 480, 2109 Melena et al. 2008; Kudryavtseva et al. 2012). The on-sky Eisenhauer F., Quirrenbach A., Zinnecker H., Genzel R., 1998, pattern of these ejections comes as a surprise in that 7 are ApJ, 498, 278 arranged in a partial ring of radii spanning 9–18 arcmin, Ekstr¨omS., et al., 2012, A&A, 537, A146 favouring the south. Radial velocities are needed to begin Evans C. J., et al., 2011, A&A, 530, A108 to add the third dimension. It is hard to see how this pat- FiguerˆedoE., Blum R. D., Damineli A., Conti P. S., 2002,AJ, tern would arise from a cloud-cloud collision, given what we 124, 2739 know about the placement of molecular clouds in the area Fujii M. S., Portegies Zwart S., 2011, Science, 334, 1380 Fujii M. S., Portegies Zwart S., 2013, MNRAS, 430, 1018 (Fukui et al. 2014). In this respect NGC 3603 is different Fukui Y., et al., 2014, ApJ, 780, 36 from Westerlund 2, where the O-star ejections are aligned Gaia Collaboration Brown A. G. 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MNRAS 000, 000–000 (0000) The O star hinterland of NGC 3603 11
◦ Table A1. Cross-matched names 291◦.617, b = −0 523. Later columns present the derived relative proper motions, PMr, and impact parameters, IP . MS-II Prior names Gaia DR2 list # identifier 13089 WR 42a 5337240002035340288 13471 WR 42e, RFS 5 and 5337420974779493248 2MASS J11144550-6115001 13529 Cl* NGC 3603 MDS 76 5337418019842038912 13546 Cl* NGC 3603 MDS 7 5337418015513333888 13555 Cl* NGC 3603 MDS 3 5337418019842060928 13570 Cl* NGC 3603 Sher 23 5337418397799183872 13572 RFS 1, MTT 31 5337417985482256768 13576 Cl* NGC 3603 Sher 18 5337418015513337472 13579 Cl* NGC 3603 Sher 22 5337418019842057088 13581 Cl* NGC 3603 Sher 47 5337418015513340160 13584 Cl* NGC 3603 MTT 47 5337418191640752896 13589 RFS 2, MTT 58 5337417985482248576 13594 Cl* NGC 3603 MTT 25 5337417813683617152 13931 2MASS J11171292-6120085 5337403073354793088 13954 RFS 8 5337401724739725184
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APPENDIX A: OBJECTS IN THE LITERATURE PRIOR TO MS-II Table A1 identifies objects in the sample of 288 stars that were known before the compilation of the MS-II catalogue and Gaia DR2 release. The obects’ prior names appear in the middle column of the table and are given in the form used by SIMBAD. The entries are in order of MS-II VPHAS- OB1-nnnnn catalogue number, which in turn is ordered by Galactic longitude. The unique identifier for the Gaia DR2 cross-match is also listed.
APPENDIX B: THE COMPLETE CROSS-MATCHED SAMPLE Table B1 lists the MS-II and Gaia DR2 identifiers along with sky positions, log Teff , extinction A0 (mag) from MS-II of all 288 stars making up the main sample discussed in this paper. For convenience, 2MASS K magnitude is also cited (column 6). The radius in column 7 is the angular distance from the adopted cluster centre, at Galactic coordinates, ` =
MNRAS 000, 000–000 (0000) 12 J. E. Drew et al 8.07 7.43 3.18 5.35 6.83 2.69 6.48 4.70 5.93 9.46 3.26 6.68 10.74 31.68 8.24 4.70 2.88 13.60 5.15 2.60 1.52 2.34 22.27 7.05 1.50 5.02 34.91 9.38 3.15 6.75 28.55 4.37 4.97 1.99 5.11 12.00 5.59 4.40 32.71 12.08 7.12 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± IP | 0.03 10.54 0.030.03 16.49 43.34 0.020.03 50.20 0.03 7.35 29.08 0.02 34.80 0.02 39.09 0.02 33.77 0.030.02 7.91 0.07 5.19 21.11 0.04 28.67 0.02 31.59 0.030.03 29.73 11.39 0.03 12.51 0.030.02 13.45 9.04 0.020.03 40.86 41.55 0.04 19.07 0.020.03 48.90 18.98 0.02 36.31 0.03 50.81 0.03 2.13 0.060.02 22.12 20.27 0.020.02 34.23 0.02 33.32 7.06 0.03 12.76 0.020.03 17.14 23.60 0.02 20.59 0.02 12.59 0.020.02 24.52 0.02 19.73 0.41 0.03 27.68 r ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± PM | 0.05 0.36 0.06 0.14 0.06 0.56 0.06 0.27 0.05 0.03 0.04 0.39 0.05 0.30 0.06 0.88 0.04 0.28 0.05 0.07 0.04 0.21 0.040.05 0.14 0.14 0.05 0.51 0.04 0.03 0.040.04 0.28 0.22 0.05 0.38 0.05 0.31 0.07 0.45 0.05 0.57 0.05 0.31 0.05 0.32 0.050.05 0.23 0.12 0.44 1.07 0.08 0.36 0.04 0.41 0.05 0.28 0.05 0.27 0.04 0.11 0.08 0.25 0.05 0.26 0.06 0.66 0.11 0.14 0.05 0.42 0.06 0.02 0.04 0.15 0.05 0.23 0.04 0.27 0.05 0.29 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± mas/yr mas/yr arcmin b µ r PM 0.05 0.19 0.05 0.11 0.07 0.10 0.06 -0.11 0.05 0.04 0.04 0.24 0.050.04 0.10 0.15 0.17 0.19 0.08 0.13 0.04 0.33 0.06 0.22 0.040.05 -0.19 0.05 0.04 0.10 0.05 -0.09 0.060.09 -0.28 0.17 0.04 0.06 0.050.06 -0.12 0.17 0.040.13 -0.21 0.10 0.05 0.42 0.040.06 -0.18 0.02 0.040.05 -0.10 -0.01 0.05 0.04 0.050.05 -0.01 0.15 0.04 0.16 0.040.05 -0.02 0.27 0.04 -0.06 0.05 -0.14 0.06 -0.14 0.04 0.52 0.05 -0.01 0.06 -0.04 0.04 -0.15 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± mas/yr ∗ `, µ Parameters of the full sample. radius DR2 Name Table B1: K 0 A eff T 12469 11:09:48.23 -60:51:53.28 4.46 5.33 10.72 45.26 5337257555529491456 0.33 12476 11:09:44.95 -60:53:22.19 4.53 4.93 11.45 44.83 5337257422423768064 -0.33 1249812499 11:09:43.62 11:07:31.43 -60:55:35.1412517 -61:33:38.67 4.56 11:08:31.01 4.54 -61:17:58.25 6.34 3.71 9.62 4.53 12.03 43.90 5.85 57.37 12.20 5337255871902117120 5337165063445617280 47.60 0.01 -0.29 5337267455469411584 -0.44 12503 11:09:28.7912550 -61:00:08.74 11:09:11.90 4.47 -61:09:13.80 4.18 4.50 11.65 3.83 43.63 12.54 5337296248933283328 43.21 -0.55 5337293465794355072 0.22 12561 11:08:01.33 -61:31:10.69 4.47 3.43 12.91 53.25 5337165407043165440 -0.30 12564 11:09:37.18 -61:03:57.00 4.53 3.99 11.45 41.42 5337248690716344704 -0.21 1258412589 11:10:27.6612594 11:10:30.58 -60:50:32.58 11:11:25.30 -60:50:02.55 4.46 -60:34:04.61 4.52 5.68 4.63 5.33 10.89 7.67 10.65 42.07 12.39 42.10 5337632355894016896 49.51 5337632458973245952 -0.21 5337640567872208512 -0.41 -1.05 12615 11:09:14.33 -61:14:39.87 4.55 5.96 12.74 42.39 5337222749113282432 -0.33 12641 11:10:03.40 -61:03:07.50 4.61 4.02 11.63 38.67 5337248214013314048 -0.26 12650 11:10:13.89 -61:01:46.21 4.51 4.58 12.36 37.96 5337254158248689280 -0.17 1265912661 11:09:12.69 11:09:58.27 -61:20:34.6312706 -61:07:55.21 4.4612710 11:10:38.75 4.49 11:09:22.36 -61:00:44.42 2.94 -61:23:16.87 4.91 11.45 4.47 12.14 4.50 42.79 4.62 37.95 5337220481370328320 3.73 12.22 5337247522488856832 -0.20 11.54 35.61 -0.26 42.02 5337254433126814080 5337219798508173440 0.03 -0.04 12693 11:10:33.58 -61:01:29.6112724 4.5212729 11:12:02.02 11:10:56.54 -60:38:32.77 5.05 -60:58:30.28 10.71 4.53 4.47 35.87 5.59 5337254330047418880 6.11 11.75 -0.38 12.19 43.34 34.73 5337639021684372608 5337253093096924288 -0.11 -0.19 12733 11:08:28.75 -61:41:33.18 4.47 5.65 11.07 54.12 5337115138740964352 -0.25 1273612754 11:09:27.91 11:08:28.87 -61:24:57.75 -61:43:39.84 4.47 4.48 2.1812809 5.22 11.9512813 11:11:55.30 12.07 41.69 11:11:09.25 -60:46:38.42 55.13 -61:00:50.84 5337218939514718976 4.56 5337114554625407232 -0.87 4.57 -0.64 4.43 7.41 10.93 12.28 37.13 32.25 5337636650862110080 5337252783859458048 -0.18 -0.09 12784 11:10:05.83 -61:17:26.6512807 4.63 11:11:55.61 -60:46:28.71 4.5312816 11.60 4.4812820 11:10:22.46 36.20 11:12:04.15 -61:14:45.52 4.50 -60:44:48.36 5337221443447103744 12.59 4.52 -0.04 4.46 37.23 3.61 5337636685221851776 4.70 11.81 12.93 0.06 34.19 37.95 5337242166699727232 5337636994459558016 -0.12 -0.01 1280012803 11:11:43.24 11:10:30.99 -60:49:56.33 -61:11:25.96 4.59 4.61 4.12 4.36 11.0212821 9.66 35.59 11:10:32.91 -61:12:06.90 5337630221251708160 33.45 -0.10 5337244193924127744 4.61 -0.14 4.12 11.46 33.14 5337244125204652160 -0.15 1282712829 11:09:46.16 11:11:00.36 -61:26:19.00 -61:04:48.68 4.60 4.47 4.87 4.29 8.93 11.95 39.89 31.61 5337218664636870400 5337250992822502912 -0.51 -0.18 12841 11:10:41.23 -61:11:11.1312884 4.5112911 11:10:34.23 11:11:18.22 -61:16:21.47 3.77 -61:06:29.10 11.98 4.58 4.51 32.27 4.16 5337244056485219072 4.76 11.97 -0.22 12.08 32.76 29.02 5337241891821629184 5337250172519332864 -0.02 -0.10 1284712862 11:10:56.47 11:10:44.82 -61:07:09.35 -61:11:46.10 4.58 4.52 4.56 3.92 11.24 11.11 31.32 31.76 5337250477426363264 5337244056485231360 0.23 -0.21 list # hh:mm:ss dd:mm:ss mag mag arcmin MS-II RA,Dec J2000 log
MNRAS 000, 000–000 (0000) The O star hinterland of NGC 3603 13 0.84 1.79 5.00 18.65 2.18 19.03 9.82 1.93 6.49 0.90 1.64 10.17 8.29 5.12 5.49 8.15 6.12 2.88 0.49 0.53 1.36 0.35 8.49 1.57 3.65 1.67 2.36 8.32 14.68 13.00 9.39 6.21 10.07 11.71 17.80 4.49 1.20 2.02 11.75 10.12 3.56 9.82 7.80 8.29 7.11 11.10 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 22.21 0.03 23.43 0.03 28.99 0.02 20.61 0.070.03 36.32 6.36 0.02 24.03 0.04 12.04 0.020.05 5.68 3.92 0.070.04 24.08 27.99 0.060.05 6.65 3.73 0.02 36.13 0.02 34.78 0.060.03 15.15 0.05 7.70 0.03 9.75 25.53 0.050.04 8.48 11.18 0.04 18.90 0.03 16.30 0.03 4.74 0.03 19.24 0.020.02 29.33 23.89 0.020.04 7.72 0.03 2.06 0.02 4.78 0.03 44.82 19.67 0.02 34.04 0.030.05 6.79 5.42 0.03 12.36 0.02 4.19 0.030.02 0.52 31.39 0.030.03 6.86 9.20 0.020.02 36.40 8.76 0.030.02 39.96 5.97 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.04 1.26 0.05 0.27 0.120.06 2.12 0.95 0.04 0.31 0.08 0.13 0.06 0.24 0.05 0.26 0.050.04 0.45 1.98 0.04 0.17 0.06 0.52 0.05 0.08 0.04 0.20 0.06 0.16 0.04 0.12 0.04 0.08 0.05 0.81 0.05 0.07 0.05 0.05 0.08 0.26 0.09 0.22 0.13 1.58 0.110.09 0.29 0.27 0.04 0.84 0.04 0.44 0.13 0.38 0.090.06 0.30 0.11 0.110.07 0.34 0.41 0.08 0.29 0.06 0.13 0.06 0.15 0.080.04 1.43 0.04 0.34 0.91 0.04 0.22 0.10 0.30 0.06 0.24 0.060.04 0.16 0.39 0.06 0.18 0.04 0.25 0.05 0.31 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.04 -1.10 0.05 -0.02 0.07 0.12 0.10 0.09 0.06 -0.30 0.110.09 0.06 0.04 0.01 -0.22 0.05 0.28 0.05 0.16 0.09 0.22 0.100.08 0.28 0.23 0.08 0.28 0.060.05 0.09 -0.11 0.080.05 0.86 0.05 0.12 0.21 0.04 -0.28 0.06 -0.07 0.060.05 0.05 0.14 0.05 0.09 0.05 -0.06 0.04 -0.03 0.05 0.20 0.05 0.06 0.05 0.01 0.15 -0.33 0.14 0.63 0.07 -0.13 0.14 0.33 0.06 0.11 0.07 -0.02 0.06 0.14 0.04 0.02 0.04 0.15 0.05 -0.41 0.07 0.23 0.05 -0.11 0.070.05 0.11 -0.01 0.04 0.19 0.04 -0.02 0.07 -0.02 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 12913 11:11:05.34 -61:10:32.63 4.58 4.05 11.34 29.50 5337243678528184704 -0.62 12917 11:12:17.17 -60:49:21.69 4.51 6.59 10.57 33.34 5337624556233014912 0.79 12921 11:10:45.46 -61:17:18.93 4.57 3.78 12.88 31.441299412997 11:10:08.69 5337241823102189056 11:12:39.90 -61:34:20.94 0.03 -60:49:44.34 4.47 4.50 3.97 5.90 12.30 10.15 40.26 31.41 5337208872110638208 5337624418794057344 -0.27 0.04 12935 11:11:35.25 -61:04:00.09 4.471297712990 11:12:03.85 5.9012992 11:13:48.80 -60:59:12.85 11.51 11:10:56.23 -60:27:56.58 4.56 28.03 -61:20:18.53 4.4613005 5337251649988151168 7.13 4.62 11:12:34.24 -0.23 7.16 12.03 -60:52:13.14 6.76 12.48 27.52 10.69 4.50 48.63 5337615897578294528 30.44 5337658945999980672 -0.20 8.73 5337240826669573504 11.54 2.10 -0.90 29.81 5337618371479573760 1.44 1294512953 11:12:11.2912967 11:11:50.93 -60:54:02.54 11:09:49.61 -61:00:45.33 4.52 -61:37:56.28 4.59 8.25 4.58 7.14 11.82 3.90 11.11 30.27 11.72 27.9313015 5337617993522362496 43.9713037 11:11:01.32 5337240517431518208 -0.28 11:10:22.28 -61:20:35.69 5337206909279575296 -0.27 -61:33:54.80 -0.22 4.57 4.62 7.59 4.93 10.57 11.22 29.88 38.63 5337240654870882048 5337208459793805696 0.02 -0.79 13047 11:10:31.08 -61:32:34.96 4.64 4.79 11.35 37.09 5337208562873277056 -0.41 13051 11:11:25.7413061 -61:16:48.3913076 11:12:37.07 4.56 11:13:03.07 -60:56:12.96 -60:49:25.53 7.73 4.57 12.73 4.52 7.66 26.59 5.20 11.04 5337230999783409024 12.14 26.54 0.20 30.18 5337617065771678592 5337623834678486656 -0.21 0.01 13057 11:11:42.33 -61:12:30.1113088 4.4613089 11:13:04.05 11:12:15.74 -60:50:25.00 5.39 -61:05:04.81 12.48 4.54 4.49 24.79 7.53 5337231652618506496 7.12 12.20 10.81 0.24 29.27 23.16 5337623800281807744 5337240002035340288 -0.20 -0.34 13093 11:12:38.05 -60:58:47.65 4.54 7.03 10.72 24.62 5337615382182127232 -0.09 1309713098 11:13:04.6813099 11:10:40.50 -60:51:02.87 11:11:53.97 -61:34:02.57 4.58 -61:12:40.93 4.55 5.77 4.51 4.41 11.83 5.90 12.09 28.68 11.71 36.79 5337623422361651584 23.38 5337208322354870656 -0.09 5337237321975474304 -0.24 0.05 1328013285 11:13:42.8913288 11:13:12.38 -61:03:07.60 11:15:34.82 -61:13:05.94 4.58 -60:29:09.83 4.54 6.81 4.56 4.41 11.50 4.13 12.23 16.09 11.21 13.99 5337612495964116096 46.60 5337235084263308544 -1.14 5337561952809554944 -0.33 0.91 13118 11:13:40.38 -60:43:13.40 4.54 4.68 10.81 34.061320413209 11:13:14.37 533764658082764505613212 11:11:10.66 -60:58:59.15 0.17 13218 11:11:22.13 -61:37:00.61 4.53 11:11:43.33 -61:33:43.61 4.49 -61:28:54.00 7.49 4.62 4.39 12.51 4.5613273 3.83 12.51 21.48 11:13:21.01 6.60 10.92 35.40 -61:08:27.84 5337613728578814976 11.02 32.39 5337196227726228480 -0.22 4.46 27.7413305 5337202240680675200 0.19 11:14:25.65 5337203683789789824 -1.96 4.92 -60:54:17.61 11.52 0.05 4.49 14.62 5337610331300437248 6.61 10.92 0.13 21.91 5337433344286091648 -0.51 1312613129 11:12:42.08 11:11:02.93 -61:01:50.69 -61:31:26.80 4.44 4.5113187 5.4613198 11:12:26.02 4.00 12.31 11:12:27.83 -61:12:00.83 11.95 22.25 -61:12:24.53 4.53 33.19 5337614626267827200 4.57 5337202962235197696 -0.15 5.4613220 -0.36 5.32 12.48 11:14:36.25 12.09 19.6813244 -60:36:25.96 19.39 11:12:53.12 5337236806579480192 4.44 -61:12:11.67 5337236806579471616 0.14 4.12 0.08 4.58 12.00 5.12 39.38 10.02 5337653968171872640 16.44 0.16 5337235329110793472 0.19 13158 11:10:38.9413178 -61:41:08.76 11:12:23.19 4.45 -61:12:18.09 4.11 4.44 12.40 5.58 40.90 12.17 5337205951532783488 19.9613225 -0.30 11:12:54.71 5337236772219725312 -61:08:33.81 0.16 4.44 4.40 11.65 17.40 5337235947586199296 -0.10 13161 11:12:25.39 -61:09:52.60 4.50 4.82 10.32 20.26 5337237150176932352 -0.08
MNRAS 000, 000–000 (0000) 14 J. E. Drew et al 2.15 0.23 9.22 0.16 0.08 5.47 0.20 0.49 0.90 0.72 0.15 0.20 2.07 0.56 0.41 1.35 1.32 1.19 1.33 0.64 1.28 0.03 2.89 2.11 2.38 2.78 1.21 3.35 1.05 1.38 1.67 6.17 1.37 1.81 8.02 2.74 1.46 1.97 1.38 3.36 2.52 1.22 2.55 10.07 0.62 3.33 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.05 25.63 0.020.04 0.77 0.50 0.050.02 0.63 0.03 0.59 0.03 1.67 1.04 0.020.04 1.53 0.03 1.62 0.75 0.070.03 0.93 0.46 0.03 0.28 0.030.04 9.23 0.05 6.63 0.06 5.94 0.02 6.65 4.96 0.080.02 5.27 3.26 0.050.05 4.14 4.21 0.05 2.51 0.03 11.86 0.03 0.28 0.03 3.10 0.06 5.13 0.030.03 1.25 4.45 0.040.03 15.67 1.16 0.060.05 8.87 31.78 0.03 3.40 0.02 0.14 0.020.06 3.48 0.03 6.54 3.95 0.020.02 1.75 0.02 2.87 11.34 0.030.03 8.11 0.03 3.54 0.02 16.08 0.27 0.02 8.52 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.08 0.68 0.05 0.12 0.07 0.11 0.11 0.27 0.06 0.12 0.05 0.37 0.11 0.21 0.08 0.11 0.08 0.06 0.05 0.31 0.05 0.87 0.05 0.25 0.06 0.08 0.070.05 0.04 0.24 0.09 0.19 0.05 0.13 0.04 0.30 0.04 0.17 0.05 0.21 0.04 0.85 0.06 0.10 0.040.07 0.08 0.05 0.31 0.31 0.050.07 0.47 0.04 0.17 0.09 0.05 0.19 0.070.09 0.31 0.09 0.34 0.04 0.36 0.16 0.04 0.95 0.08 0.36 0.09 0.22 0.06 0.46 0.08 0.43 0.050.10 0.80 0.05 0.52 0.13 0.040.05 0.36 0.18 0.050.06 0.05 0.45 0.04 0.13 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.040.08 0.02 0.29 0.110.05 -0.27 0.47 0.05 -0.12 0.060.10 0.13 -0.01 0.15 -0.11 0.110.12 0.27 0.05 0.16 0.07 0.15 -0.00 0.050.05 0.94 -0.30 0.11 0.04 0.11 -0.04 0.050.13 -0.15 0.06 0.12 -0.80 0.070.06 0.45 -0.13 0.07 -0.03 0.10 0.12 0.05 -0.13 0.12 -0.07 0.05 0.71 0.06 0.09 0.04 0.02 0.04 -0.07 0.05 -0.00 0.05 0.06 0.04 -0.36 0.07 0.02 0.06 0.25 0.090.06 0.15 0.05 0.08 0.04 0.17 -0.04 0.11 -0.04 0.08 -0.04 0.12 0.07 0.06 -0.01 0.06 0.17 0.060.06 0.03 0.44 0.06 -0.10 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 13325 11:13:34.84 -61:13:22.12 4.52 4.46 11.57 11.29 5337234195239491200 -0.17 13512 11:15:01.35 -61:15:01.21 4.64 6.56 11.34 0.89 5337418088561808000 0.10 1349213493 11:14:55.2513494 11:14:52.88 -61:15:20.6113495 11:14:56.27 -61:16:07.11 4.6313500 11:13:29.60 -61:15:12.23 4.6213503 11:15:48.45 -61:41:35.96 5.29 4.6213509 11:15:02.30 -60:59:15.38 5.39 10.37 4.5113511 11:15:00.69 -61:13:51.94 5.97 12.34 4.59 11:14:59.78 1.41 -61:15:01.80 5.84 11.26 4.60 1.74 -61:15:24.67 5.12 12.96 5337418054201746432 4.62 1.33 7.54 12.13 5337417951098962560 4.64 -0.08 28.44 6.16 10.94 5337418054201754752 -0.11 17.14 5337010749528525440 5.25 10.65 0.19 1.85 5337429113701924736 -0.63 11.35 0.95 -0.08 5337418500878432128 0.87 5337418088538280064 0.07 5337418054202067584 0.07 -0.05 1348613490 11:15:00.35 11:14:57.32 -61:12:29.87 -61:14:39.25 4.64 4.62 6.63 7.56 10.58 11.06 3.23 1.50 5337418603957679104 5337418088561534848 -0.13 -0.11 13472 11:14:46.08 -61:14:50.64 4.52 6.99 12.66 2.61 5337421009139238912 -0.25 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MNRAS 000, 000–000 (0000) The O star hinterland of NGC 3603 15 3.42 1.75 9.12 0.66 0.30 0.12 0.15 0.40 0.39 0.12 0.90 0.00 0.42 0.01 0.52 0.04 0.25 0.14 0.05 0.21 0.05 0.81 0.54 0.45 0.09 0.19 0.02 0.46 0.07 0.90 0.04 0.61 0.09 0.18 0.18 0.04 0.06 0.79 0.03 0.56 0.05 0.29 0.14 0.19 1.18 0.16 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.07 16.48 0.04 1.40 0.060.02 1.40 0.03 0.55 0.05 0.02 0.51 0.10 1.58 0.020.02 0.48 0.02 0.19 0.02 0.69 0.03 1.12 0.03 0.56 0.02 0.47 0.60 0.04 0.27 0.03 0.30 0.030.03 0.28 0.40 0.030.03 0.28 1.39 0.04 0.02 0.05 1.81 0.02 0.87 0.03 0.12 0.020.03 0.23 0.03 2.99 0.21 0.04 0.41 0.05 30.41 0.030.05 0.20 0.02 1.51 0.28 0.02 0.14 0.02 0.01 0.020.04 0.33 0.04 1.04 0.02 1.12 0.07 0.18 1.93 0.03 14.30 0.04 0.68 0.040.07 0.44 0.13 0.050.05 0.84 1.78 0.03 0.56 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.13 0.65 0.08 0.14 0.11 0.26 0.14 0.18 0.04 0.07 0.08 0.47 0.05 0.16 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9.28 5.29 9.08 10.86 3.05 0.39 0.45 5337419836572100096 5337418397799183872 -0.08 5337418015513335168 0.26 0.12 13560 11:15:08.19 -61:15:47.21 4.61 5.12 9.64 0.23 5337418015513335552 -0.02 1355013555 11:15:13.5213556 11:15:08.90 -61:13:46.95 11:15:11.55 -61:15:27.22 4.60 -61:14:40.48 4.62 8.21 4.61 4.78 10.59 7.65 10.93 2.02 11.22 0.32 5337418530902030720 1.12 5337418019842060928 0.23 5337418432158952576 -0.07 0.02 1354213546 11:13:25.9013549 11:15:07.82 -61:45:57.88 11:15:06.66 -61:15:27.84 4.60 -61:15:52.68 4.60 6.19 4.59 5.19 12.80 5.42 9.95 32.63 11.91 5337008692248970496 0.21 0.24 -0.71 5337418015513333888 5337418019842021120 0.02 -0.22 1353013532 11:15:07.7113533 11:15:13.36 -61:14:35.4713534 11:15:05.66 -61:13:03.50 4.6313541 11:15:11.51 -61:15:26.93 4.55 11:15:06.61 -61:13:38.67 7.22 4.58 -61:15:23.71 7.60 11.72 4.48 5.04 11.43 4.59 1.05 7.79 11.51 2.70 4.92 12.32 5337418397776101376 0.23 11.27 5337418569580191872 0.22 2.07 5337418019842034432 0.12 0.24 5337418530903538432 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MNRAS 000, 000–000 (0000) 16 J. E. Drew et al 17.20 0.54 1.09 1.26 4.80 2.07 1.66 0.10 1.59 1.02 1.50 1.94 1.33 0.22 1.17 0.29 0.41 1.00 0.74 1.22 1.09 1.22 0.03 0.23 1.56 1.49 1.58 1.25 2.90 0.72 0.66 0.75 1.11 1.24 1.21 1.26 0.08 0.37 0.61 0.46 0.80 1.18 0.38 0.38 0.36 0.31 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.040.04 2.17 0.07 8.19 0.04 3.10 0.06 1.41 0.03 1.58 22.67 0.060.04 2.59 0.05 1.28 0.04 0.65 0.82 0.05 3.44 0.020.06 26.78 0.56 0.040.04 7.95 1.52 0.03 2.58 0.02 0.55 0.02 7.89 0.040.04 1.97 1.31 0.030.03 1.17 0.03 2.28 2.20 0.030.03 8.83 0.03 0.69 0.02 0.22 3.18 0.040.03 0.44 3.73 0.060.02 1.22 0.05 1.42 0.04 0.85 0.04 0.74 0.04 1.03 0.26 0.06 1.15 0.020.06 1.17 0.05 4.96 0.03 1.02 0.05 0.76 0.07 1.68 1.75 0.02 0.67 0.04 1.12 0.04 0.54 0.04 1.36 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.07 0.21 0.13 1.28 0.040.10 0.77 0.31 0.07 0.33 0.06 0.19 0.04 0.27 0.04 0.35 0.06 0.20 0.07 0.13 0.05 0.26 0.07 0.10 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